论文标题
三角形银河系中恒星形成和反馈的云规模无线电调查M 33：VLA观察
Cloud-scale Radio Surveys of Star Formation and Feedback in Triangulum Galaxy M 33: VLA Observations
论文作者
论文摘要
研究大型恒星形成与星际介质（ISM）之间的相互作用至关重要，这对于了解星系的演变至关重要。无线电连续体（RC）发射是巨大恒星形成和星际介质的能量成分的无灭绝示踪剂。我们提出了一项对本地组星系M 33的多波段无线电连续调查，低于〜30 pc的线性分辨率，使用Karl G. Jansky非常大的阵列（VLA）观察到。我们使用结构分解来校准恒星形成速率的表面密度，并研究弥散发射对这种校准的影响。还研究了星际介质的不同阶段与巨大恒星形成的影响之间的相关性。尺寸<〜200 PC的无线电源约占M 33的内部18'x 18'（或4KPC x 4KPC）磁盘的总RC排放量的36％（46％）。非热光谱索引在cosmic ray Elect} cosmic ray Elect} compant cossmic ray Elect} compant} compant} compant} compant} floptert platter。双模式关系后，磁场强度还随着恒星形式的增加而增加，这表明小规模的湍流发电机在较高的亮度和恒星形态速率下更有效地起作用。尽管在星形区域中的相关性更紧密，但非热发射也与ISM中更静止的分子气体相关。当不排除弥漫性结构时，在M 33中存在几乎线性的分子形成定律。巨大的恒星形成扩大了磁场，并增加了高能宇宙射线电子的数量，这可以帮助风和流出。
Studying the interplay between massive star formation and the interstellar medium (ISM) is paramount to understand the evolution of galaxies. Radio continuum (RC) emission serves as an extinction-free tracer of both massive star formation and the energetic components of the interstellar medium. We present a multi-band radio continuum survey of the local group galaxy M 33 down to ~30 pc linear resolution observed with the Karl G. Jansky Very Large Array (VLA). We calibrate the star-formation rate surface density and investigate the impact of diffuse emission on this calibration using a structural decomposition. Separating the thermal and nonthermal emission components, the correlation between different phases of the interstellar medium and the impact of massive star formation are also investigated. Radio sources with sizes <~ 200 pc constitute about 36% (46%) of the total RC emission at 1.5 GHz (6.3 GHz) in the inner 18' x 18' (or 4kpc x 4kpc) disk of M 33. The nonthermal spectral index becomes flatter with increasing star-formation rate surface density, indicating the escape of cosmic ray electrons {from their birth places}. The magnetic field strength also increases with star-formation rate following a bi-modal relation, indicating that the small-scale turbulent dynamo acts more efficiently at higher luminosities and star-formation rates. Although the correlations are tighter in star-forming regions, the nonthermal emission is correlated also with the more quiescent molecular gas in the ISM. An almost linear molecular star-formation law exists in M 33 when excluding diffuse structures. Massive star formation amplifies the magnetic field and increases the number of high-energy cosmic ray electrons, which can help the onset of winds and outflows.
